Martian Gullies: Produced by Fluidization Of

Martian gullies: Produced by fluidization of dry material Yolanda Cedillo-Flores, a,b and aHéctor Javier Durand-Manterola [email protected] , [email protected] a Departamento de Física Espacial, Instituto de Geofísica, Universidad Nacional Autónoma de México. UNAM. Coyoacan C.P 04510. D.F. Mexico. b Posgrado de Geografía, Facultad de Filosofía y Letras, Universidad Nacional Autónoma de México. Circuito Interior. Ciudad Universitaria s/n. C.P 04510. D.F. Mexico. (Submitted to Planetary and Space Science) Abstract Context: The gullies on Mars were discovered in the year 1999. Their aspect suggests that they had been formed recently on Martian slopes. Since then several hypotheses have appeared trying to explain the presence of these gullies. The main hypotheses are the ones which suggest that some liquid, water or CO2, was responsible for modeling the gullies and ones that propose dry flows as the modeling agents. Objective: The aim of this work is to develop an alternative hypothetical mechanism of formation of Martian gullies. Method: Our model proposes that the Martian gullies were formed as a result of a fluidization process of the material deposited on the slopes of the impact craters, plateaux and other geomorphologic structures. This fluidization is caused by the sublimation of carbon dioxide ice deposited in the form of snow, due to the daily and seasonal temperature changes. We also present the results of an experimental simulation. Results: Structures similar to the Martian gullies were reproduced using the air injection mechanism, as a substitute to gaseous CO2, on a sandy slope. The Reynolds number for our experimental flow and for the flow in the Martian gullies was calculated and we found that they are of the same order, whilst the water flows have much higher Reynolds numbers. Taking into account the current environmental conditions for Mars, from our results it may be suggested that this mechanism is the possible modeling agent for the Martian gullies. Two of the most important characteristics of the proposed model are: a) It offers a simple explanation of how recurrent fluidization events occur in the same place, a necessary recurrence of the formation of a gully, offering a recharging mechanism for the system after every fluidization event, and b) It considers the formation of gullies possible even in angles smaller than the angle of repose. These characteristics of the model solve these two problems present in current theories. Key Words: Martian gullies, fluidization, Martian geology 1 Introduction: In the year 1999, Malin and Edgett discovered gullies in the images from planet Mars, obtained by the Mars Global Surveyor (MGS) spacecraft, which had the appearance of being formed recently on Martian slopes. (Malin and Edgett, 2000; Hartmann, 2003). The discovery of Martian gullies immediately generated the following questions: How did these gullies form? What structure did they have? How old were they? On what type of geological material were they formed? What was the geographic distribution of these features? Gullies are landforms formed over several types of slopes. The Martian gullies normally exhibit the three characteristic forms present in terrestrial gullies: alcove, channel and apron or debris cone, although not all the gullies present these three forms or features. The channels extend from the base of the alcove towards the lower part of the slope. Some of the channels gradually fade at the foot of the slope. These features are located in the relief of the Noachian, Hesperian and Amazonian eras in both hemispheres, north and south, as well as in several latitudes. However the gullies predominate in mid-latitudes, between the 30º and 60º (Heldmann and Mellon, 2004, Mellon and Phillips, 2001; Bridges and Laqckner, 2006). Checking images obtained from the cameras of three NASA spacecrafts: Martian Orbiter Camera (MOC), Mars Global Surveyor (MGS), Thermal Emission Imaging System (THEMIS), from the Mars Odissey spacecraft, and High Resolution Imaging Science Experiment (HiRISE), from the Reconnaissance Orbiter spacecraft, as well as some images obtained by the Mars Express spacecraft, from the ESA, (European Spatial Agency) we led to the same conclusions. Several explanations of the origin of the gullies have emerged which can be separated into two groups: theories which invoke the presence of a fluid (generally water) and theories which proposes the existence of the gullies as a result of dry material avalanches. The first theories include the existence of aquifers, (Mellon and Phillips, 2001; Frey et al, 2004; Costard et al, 2002; Christensen et al., 2003; Mangold et al., 2003), highly saline water (Doran y Forman, 2000; Knauth et al., 2000; Wynn-Williams et al., 2001; Knauth and Burt, 2002; Heldmann et al., 2005) or liquid carbon dioxide (Musselwhite et al, 2001; Draper et al., 2000 y Hoffman, 2001 a and b). The second group of theories refers to avalanches of deposited granular material by means of aeolian activity (Treiman 2003, Shinbrot, et al,. 2004). The argument for the gullies having been formed by water or liquid CO2 presents several weak points due to the pressure and temperature conditions which currently exist on Mars and the distribution of these features. In the distant past, when the atmosphere and pressure was high enough to maintain the water in a liquid state on the surface of the planet, the formation of the gullies by this liquid was feasible. However, characteristics of the gullies indicate that they are probably not that old, maybe some millions of years old. The prevailing conditions on Mars in recent millions of years make it very improbable that water is the main agent responsible for the formation of gullies. Although Lobitz et al (2001) have demonstrated that liquid water can be stable over extended areas on the surface of Mars, the excavation of gullies on rocky slopes requires several water liberation events from an aquifer and this in turn requires its own refilling mechanism. On Earth this refilling is done by rain, but this option is beyond the possibilities of the current Martian environment. On the other hand, the dry flow theory also presents weak points. Most of the gullies have been formed on slopes with inclinations smaller than the angle of repose (Heldmann y Mellon, 2004) and it is not quite clear how the dry material could have slid down under these conditions, which represents an unresolved point for the dry flow theory. Pelletier et al (2008) performed simulations and compared velocity with distance between the flow with liquid and the dry flow. The end result was that the dry flow can erode to angles smaller than 33º, whilst it preserves its momentum, but it is necessary that it commences at angles greater than 33º. In this work an alternative model is proposed to try to solve the weak points present in other hypotheses. We suggest that the Martian gullies were formed, and still are formed, by fluidization of dust and water ice accumulated on the impact crater slopes or canyons due to the sublimation of CO2 snow presents on these slopes as well. A series of experimental simulations were performed using an experimental device in order to try to reproduce analogue forms of Martian gullies. Then the results were compared. 2 Model and experimental simulation 2.1 Gullies formed by granular flows fluidized by CO2 gas. In the proposed model, the scenario is as follows: over the gullies of the impact craters, canyons and other Martian landforms, the wind deposits dust and sand. This material then slides down towards the base of the slope, the resulting erosion forms a gully. A landslide of this type, without any other help than gravity, would be impossible at angles smaller than the angle of repose. However if the CO2 or any other gas is injected into the interior of the granular mass, the grains separate and the gas flow will prevent the contact between the grains, allowing the mixture (sand+gas) to flow like a liquid on any slope (fluidization). The landslide erodes the ground forming a gully and when this is recurrent, whether it is daily or yearly or every time the planet obliquity changes, an evolution of the gullies is expected; this growth in time will dig the deepest channel. The material displaced accumulates at the base of the slopes and forms an apron of debris. This process is feasible and probable on Mars. In winter and at night, the sand transported by the wind mixes with the H2O and CO2 snow. In spring or during the day this mixture can warm up, causing the CO2 gas to elevate and flow between the grains of dust, sand and snow, resulting in the fluidization of these materials. In our model erosion speed of a slope will depends of its material. For instance, on sand dunes gullies will form after few fluidization events. On the other hand in slopes of more hardness material, thousands of events are necessary to form the structures. 2.2 Description of the experimental simulations An experimental device (Fig.1) was built, which consisted of (a) a container with dimensions of 30 cm width, 50 cm length and 30 cm height. Six kg of fine grain volcanic sand (grains between 1.2 mm and 0.03 mm) were placed within the container and used to build a slope (c). To simulate the CO2 on Mars, air at atmospheric pressure was injected through an air pump (d), via a tube (b) of 6 mm diameter and 7 cm length, within the slope. The tube was inserted at a depth of 4 cm, parallel to the slope. So that the air could be injected through the tube it was perforated every 9 mm. When pumping the air the sand bubbles.

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